The R-AXIS RAPID II Located at the Natural History Museum of Los Angeles County the Natural History Museum of L.A

Total Page:16

File Type:pdf, Size:1020Kb

The R-AXIS RAPID II Located at the Natural History Museum of Los Angeles County the Natural History Museum of L.A MATERIALS ANALYSIS eNEWSLETTER OCTOBER 2013, ISSUE 4 The R-AXIS RAPID II located at the Natural History Museum of Los Angeles County The Natural History Museum of L.A. County, 900 Exposition Blvd., Los Angeles, CA 90007, Dr. Anthony R. Kampf, Curator Emeritus The Natural History Museum of Los Angeles County opened on November 6, 1913 at Exposition Park in L.A. and has since grown to be the largest such museum in Dr. Kampf joined NHM in January 1977, after earning the western U.S. As Curator of Mineral Sciences for his Ph.D. in mineralogy and crystallography from the University of Chicago. The current mineral sciences lab at NHM developed around his knowledge of mineralogy, crystal chemistry and structural crystallography. He has analyzed countless unknown minerals and described 26 new minerals between 1975 and 2008. Interestingly enough, over 100 new minerals are still found by mineralogists every year around the world. Dr. Anthony R. Kampf more than 34 years, Dr. Anthony R. Kampf was instrumental in building the museum’s extensive collection of gems and minerals, its beautiful gem and mineral exhibition, as well as performing scientific research in descriptive mineralogy and structural crystallography. Since retiring in 2011, Dr. Kampf Dr. Anthony R. Kampf and his R-AXIS RAPID II has continued his research as Curator Emeritus. Copyright © 2013 – Rigaku Corporation and its Global Subsidiaries. All Rights Reserved. | 1 The R-AXIS RAPID II, one of Rigaku’s curved imaging to investigate by conventional XRD and so usually have plate X-ray diffraction systems, was installed at NHM by to be studied using EBSD (electron backscatter Dr. Kampf in November 2007. He needed to replace diffraction). The krotite in this inclusion was large enough obsolete powder and single-crystal XRD systems that that I was able to use the RAPID II. I first mounted the were film-based. He chose the R-AXIS RAPID II because entire microscope slide on the RAPID and recorded the it can measure both powder and single-crystal data. powder diffraction pattern of the krotite using reflection When Dr. Kampf is faced with an unknown mineral mode. I then succeeded in extracting a 110 x 60 x 20 µm phase, he first obtains an X-ray powder diffraction pattern crystal fragment, from which I collected single-crystal and performs a search against a database of known structure data. I obtained an excellent structure minerals. If the X-ray powder pattern does not match a refinement with R1 = 1.6%. For me the charm of scientific known mineral and occurs in crystals of sufficient size mineralogy comes from making discoveries, each of and quality, Dr. Kampf then pursues a single-crystal which helps us to understand the world around us a little study and structure analysis. The dual-purpose better. I was particularly happy to be a part of the team functionality of the R-AXIS RAPID II (powder and single that worked on krotite because it adds to our crystal) has proven ideal to Dr. Kampf’s work, allowing understanding of how our solar system formed. The him to quickly and easily switch between the two special feeling that comes from making a discovery is methods. In the 6 years since obtaining the R-AXIS what has kept me involved in research even after RAPID II, Dr. Kampf has characterized more than 75 new retirement. In fact, the only reason that I retired was so minerals, three times the number that he had that I could spend more time doing research and using characterized in the previous 33 years! the R-AXIS RAPID II, which has proven to be an essential and irreplaceable research tool.” From left to right, Collections Manager Alyssa Morgan, Associate Curator Eloïse Gaillou,and Dr. Anthony R. Kampf One of his signature XRD studies with the R-AXIS RAPID II was his work on the new mineral krotite in 2011 (American Mineralogist, Volume 96, pages 709–715, 2011). This phase is considered one of the earliest formed in our solar system. Dr. Kampf told us that the new mineral krotite, CaAl2O4, was found as the main component of a tiny inclusion in a meteorite. “Inclusions like this one are usually studied in thin- sections mounted on glass microscope slides. The phases in inclusions like this are almost always too small Copyright © 2013 – Rigaku Corporation and its Global Subsidiaries. All Rights Reserved. | 2 .
Recommended publications
  • Addibischoffite, Ca2al6al6o20, a New Calcium Aluminate Mineral from The
    1 Revision 3 2 Addibischoffite, Ca2Al6Al6O20, a new calcium aluminate mineral from 3 the Acfer 214 CH carbonaceous chondrite: A new refractory phase from 4 the solar nebula 5 Chi Ma1,*, Alexander N. Krot2, Kazuhide Nagashima2 6 1Division of Geological and Planetary Sciences, California Institute of Technology, 7 Pasadena, California 91125, USA 8 2Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, 9 Honolulu, Hawai‘i 96822, USA 10 11 ABSTRACT 12 Addibischoffite (IMA 2015-006), Ca2Al6Al6O20, is a new calcium aluminate mineral 13 that occurs with hibonite, perovskite, kushiroite, Ti-kushiroite, spinel, melilite, 14 anorthite and FeNi-metal in the core of a Ca-Al-rich inclusion (CAI) in the Acfer 15 214 CH3 carbonaceous chondrite. The mean chemical composition of type 16 addibischoffite by electron probe microanalysis is (wt%) Al2O3 44.63, CaO 15.36, 17 SiO2 14.62, V2O3 10.64, MgO 9.13, Ti2O3 4.70, FeO 0.46, total 99.55, giving rise to 18 an empirical formula of 3+ 3+ 2+ 19 (Ca2.00)(Al2.55Mg1.73V 1.08Ti 0.50Ca0.09Fe 0.05)Σ6.01(Al4.14Si1.86)O20. The general 20 formula is Ca2(Al,Mg,V,Ti)6(Al,Si)6O20. The end-member formula is Ca2Al6Al6O20. 21 Addibischoffite has the P1 aenigmatite structure with a = 10.367 Å, b = 10.756 Å, c 22 = 8.895 Å, α = 106.0°, β = 96.0°, γ = 124.7°, V = 739.7 Å3, and Z = 2, as revealed by 23 electron back-scatter diffraction. The calculated density using the measured 24 composition is 3.41 g/cm3.
    [Show full text]
  • Grossite and Hibonite Bearing Refractory Inclusions in the CO3.1 Chondrite Miller Range 090019. D. K. Ross1 and J. I. Simon2, 1U
    49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2559.pdf Grossite and Hibonite Bearing Refractory Inclusions in the CO3.1 Chondrite Miller Range 090019. D. K. Ross1 and J. I. Simon2, 1University of Texas El Paso/Jacobs Technology/NASA-JSC-ARES (2224 Bay Area Blvd. Houston TX 77058, USA ([email protected]), 2NASA-Johnson Space Center-ARES ([email protected]). Introduction: We have characterized 142 refract- finer grained particles with substantial porosity. Ongo- ory objects by EDS hyperspectral X-ray mapping in the ing reaction with nebular gases produces down-temper- CO3.1 chondrite MIL 090019-13. These include 127 ature phases partially replacing earlier formed phases Ca-Al rich inclusions (CAIs), 14 amoeboidal olivine ag- and infilling porosity, leading to densified objects. gregates (AOAs) and one Al-rich chondrule. These data Most CAIs are not fully equilibrated, but exhibit miner- are being used to reveal the mineralogy, texture and alogy reflecting a considerable range of temperature, bulk composition of these inclusions, and to identify ob- with relict phases. Hibonite is typically intergrown with, jects that represent endmembers within cogenetic popu- and partially replaced by spinel, violating the predicted lations of primitive inclusions, which will be further in- crystallization order from thermodynamic calcula- vestigated by future isotopic studies. Previous work re- tions[3], in which melilite should precede spinel crystal- lated to these refractory inclusions in this chondrite also lization. appear in [1] and [2]. Twenty six inclusions are hibonite-bearing, 18 are grossite-bearing and one inclusion is corundum-rich. In seven of these inclusions, grossite and hibonite coexist.
    [Show full text]
  • In Iron Silicide
    CALCIUM-ALUMINUM-RICH INCLUSIONS (CAIs) IN IRON SILICIDE (XIFENGITE, GUPEIITE, HAPKEITE) 76th Annual Meteoritical Society Meeting (2013) MATTER: EVIDENCE OF A COSMIC ORIGIN 5055.pdf Abstract The CAIs Mm- to cm-sized metallic particles in the subsoil of -- The iron silicides from the Chiemgau impact strewn field contain CAIs with M.A. Rappenglück the Alpine Foreland are composed of iron silicides minerals CaAl2O4, calcium monoaluminate, and Ca2Al2O5, dicalcium dialuminate. Institute for Interdisciplinary Studies, Fe3Si, mineral gupeiite, Fe5Si3, mineral xifengite, -- The monoclinic high-temperature (>1,500°C), low-pressure dimorph of CaAl2O4, Gilching, Germany, [email protected] Fe2Si, mineral hapkeite, FeSi, fersilicite, and FeSi2, mineral krotite, was first identified in a CAI from the CH chondrite NWA 470 [17] ferdisilicite, the minerals gupeiite, xifengite and and later reported [18, 19] to exist in a CAI in the carbonaceous chondrite meteorite F. Bauer 10 µm 2 µm NWA 1934. fersilicite being the main components. More peculiar Oxford Instruments GmbH Nano- Science, mineral components add to the matrix also hosting -- The orthorhombic Ca2Al2O5 dicalcium dialuminate high pressure phase with the Fig. 6. Zircon crystals obviously having impacted larger crystals of extremely pure titanium carbide, Fig. 5. Zircon crystals in iron silicide matrix. brownmillerite-type structure was established in 2000 [20] and has so far no natural Wiesbaden Germany, The white tips on the crystals have been shown a plastic or liquid iron silicide matrix that seems [email protected] mineral khamrabaevite, and silicon carbide, mineral to be uranium. to have been frozen during the disturbance. counterpart. Experimental data were 1,250°C and 2.5 GPa, and stability was reached moissanite.
    [Show full text]
  • Compiled Thesis
    SPACE ROCKS: a series of papers on METEORITES AND ASTEROIDS by Nina Louise Hooper A thesis submitted to the Department of Astronomy in partial fulfillment of the requirement for the Bachelor’s Degree with Honors Harvard College 8 April 2016 Of all investments into the future, the conquest of space demands the greatest efforts and the longest-term commitment, but it also offers the greatest reward: none less than a universe. — Daniel Christlein !ii Acknowledgements I finished this senior thesis aided by the profound effort and commitment of my thesis advisor, Martin Elvis. I am extremely grateful for him countless hours of discussions and detailed feedback on all stages of this research. I am also grateful for the remarkable people at Harvard-Smithsonian Center for Astrophysics of whom I asked many questions and who took the time to help me. Special thanks go to Warren Brown for his guidance with spectral reduction processes in IRAF, Francesca DeMeo for her assistance in the spectral classification of our Near Earth Asteroids and Samurdha Jayasinghe and for helping me write my data analysis script in python. I thank Dan Holmqvist for being an incredibly helpful and supportive presence throughout this project. I thank David Charbonneau, Alicia Soderberg and the members of my senior thesis class of astrophysics concentrators for their support, guidance and feedback throughout the past year. This research was funded in part by the Harvard Undergraduate Science Research Program. !iii Abstract The subject of this work is the compositions of asteroids and meteorites. Studies of the composition of small Solar System bodies are fundamental to theories of planet formation.
    [Show full text]
  • Template for Two-Page Abstracts in Word 97 (PC)
    STACKING DEFECTS IN SYNTHETIC AND METEORITIC HIBONITES: IMPLICATIONS FOR HIGH- TEMPERATURE PROCESSES IN THE SOLAR NEBULA. J. Han1,2, L. P. Keller2, A. J. Brearley3, and L. R. Danielson4. 1Lunar and Planetary Institute, Houston, TX 77058, USA ([email protected]), 2ARES, NASA/JSC, Houston, TX 77058, USA, 3Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM 87131, USA, 4Jacobs JETS, NASA/JSC, Houston, TX 77058, USA. Introduction: Hibonite (CaAl12O19) is a primary, with uniform d-spacings, indicative of the presence of highly refractory phase occurring in many Ca-Al-rich ordered, stoichiometric hibonite. Most hibonite crystals inclusions (CAIs) from different chondrite groups, ex- are free of defects, but a few grains contain a very low cept CI chondrites [1]. Hibonite is predicted to be one density of stacking defects parallel to the c axis. Lattice of the earliest minerals to condense during cooling of fringe images of hibonite grains show isolated, single the solar nebula at higher temperatures than any other layers of 2.6 nm (001) spacing within ordered hibonite major CAI mineral [2]. Therefore, hibonite has great of 2.2 nm (001) spacing. Quantitative EDX analyses potential to reveal the processes and conditions of the show that hibonite grains have a uniform composition very early, high-temperature stages of the solar nebular of pure CaAl12O19, but defect-rich areas in hibonite evolution. show Ca deficiencies up to ~8 mol%. Previous microstructural studies of hibonite in CAIs and their Wark-Lovering (WL) rims showed the presence of numerous stacking defects in hibonite. These defects are interpreted as the modification of the stacking sequences of spinel and Ca-containing blocks within the ideal hexagonal hibonite structure [3,4], as shown by experimental studies of reaction-sintered ceramic CaO-Al2O3 compounds [5].
    [Show full text]
  • The Behaviour of Siderite Rocks in an Experimental Imitation of Pyrometamorphic Processes in Coal-Waste Fires: Upper and Lower Silesian Case, Poland
    minerals Article The Behaviour of Siderite Rocks in an Experimental Imitation of Pyrometamorphic Processes in Coal-Waste Fires: Upper and Lower Silesian Case, Poland Łukasz Kruszewski 1 and Justyna Ciesielczuk 2,* 1 Institute of Geological Sciences, Polish Academy of Sciences (ING PAN), Twarda 51/55, 00-818 Warszawa, Poland; [email protected] 2 Faculty of Natural Sciences, University of Silesia, B˛edzi´nska60, 41-205 Sosnowiec, Poland * Correspondence: [email protected] Received: 18 May 2020; Accepted: 26 June 2020; Published: 29 June 2020 Abstract: Little is known of the influence of fluxes on the nature and the intensity of burning in coal-waste heaps. To gain some insight, two siderite samples, one each from coal-mining waste heaps in Upper- and Lower Silesian Coal Basins (Poland), were heated under identical conditions in a thermal chamber coupled to a powder X-ray diffractometer. Differences in the behaviour of siderite phase and the products of its decomposition, mainly magnetite, wüstite, and olivine, are discussed. The waste heaps sampled underwent self-heating and self-ignition catalysed by fluxes. Though the samples are unlikely to be truly representative of the Silesian basins, the heterogeneous behaviour they displayed on heating merits description and explanation, as siderite is an important widely known flux in pyrometamorphic processes. Keywords: thermal chamber experiment; Powder X-ray Diffraction; pyrometamorphism; siderite; wüstite; magnetite; graphite 1. Introduction In coal basins in Poland, siderite occurs mainly as concretions of different sizes and shapes within mudstones, coaly shales, sandstones, and conglomerates hosting coal seams. As is common worldwide, these seams can undergo spontaneous combustion influenced by numerous external and internal factors [1–6].
    [Show full text]
  • Chance and Necessity in the Mineral Diversity of Terrestrial Planets
    295 The Canadian Mineralogist Vol. 53, pp. 295-324 (2015) DOI: 10.3749/canmin.1400086 MINERAL ECOLOGY: CHANCE AND NECESSITY IN THE MINERAL DIVERSITY OF TERRESTRIAL PLANETS § ROBERT M. HAZEN Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Road NW, Washington, DC 20015, U.S.A. EDWARD S. GREW School of Earth and Climate Sciences, University of Maine, Orono, Maine 04469, U.S.A. ROBERT T. DOWNS AND JOSHUA GOLDEN Department of Geosciences, University of Arizona, 1040 E. 4th Street, Tucson, Arizona 85721-0077, U.S.A. GRETHE HYSTAD Department of Mathematics, University of Arizona, 617 N. Santa Rita Ave., Tucson, Arizona 85721-0089, U.S.A. ABSTRACT Four factors contribute to the roles played by chance and necessity in determining mineral distribution and diversity at or near the surfaces of terrestrial planets: (1) crystal chemical characteristics; (2) mineral stability ranges; (3) the probability of occurrence for rare minerals; and (4) stellar and planetary stoichiometries in extrasolar systems. The most abundant elements generally have the largest numbers of mineral species, as modeled by relationships for Earth’s upper continental crust (E) and the Moon (M), respectively: 2 LogðNEÞ¼0:22 LogðCEÞþ1:70 ðR ¼ 0:34Þð4861 minerals; 72 elementsÞ 2 LogðNMÞ¼0:19 LogðCMÞþ0:23 ðR ¼ 0:68Þð63 minerals; 24 elementsÞ; where C is an element’s abundance in ppm and N is the number of mineral species in which that element is essential. Several elements that plot significantly below the trend for Earth’s upper continental crust (e.g., Ga, Hf, and Rb) mimic other more abundant elements and thus are less likely to form their own species.
    [Show full text]
  • An Evolutionary System of Mineralogy, Part II: Interstellar and Solar Nebula Primary Condensation Mineralogy (> 4.565
    This is a preprint, the final version is subject to change, of the American Mineralogist (MSA) Cite as Authors (Year) Title. American Mineralogist, in press. DOI: https://doi.org/10.2138/am-2020-7447 1 REVISION #2—07 May 2020—American Mineralogist 2 3 An evolutionary system of mineralogy, part II: Interstellar and solar 4 nebula primary condensation mineralogy (> 4.565 Ga) 5 1 1,* 6 SHAUNNA M. MORRISON AND ROBERT M. HAZEN 7 1Earth and Planets Laboratory, Carnegie Institution for Science, 8 5251 Broad Branch Road NW, Washington DC 20015, U. S. A. 9 10 11 ABSTRACT 12 The evolutionary system of mineralogy relies on varied physical and chemical attributes, 13 including trace elements, isotopes, solid and fluid inclusions, and other information-rich 14 characteristics, to understand processes of mineral formation and to place natural condensed 15 phases in the deep-time context of planetary evolution. Part I of this system reviewed the earliest 16 refractory phases that condense at T > 1000 K within the turbulent expanding and cooling 17 atmospheres of highly evolved stars. Part II considers the subsequent formation of primary 18 crystalline and amorphous phases by condensation in three distinct mineral-forming environments, 19 each of which increased mineralogical diversity and distribution prior to the accretion of 20 planetesimals > 4.5 billion years ago: 21 1) Interstellar molecular solids: Varied crystalline and amorphous molecular solids containing 22 primarily H, C, O, and N are observed to condense in cold, dense molecular clouds in the 23 interstellar medium (10 < T < 20 K; P < 10-13 atm). With the possible exception of some 24 nano-scale organic condensates preserved in carbonaceous meteorites, the existence of Always consult and cite the final, published document.
    [Show full text]
  • MOLLUSK SHELL) and Al2o3 POWDERS
    Ceramics-Silikáty 62 (4), 355-363 (2018) www.ceramics-silikaty.cz doi: 10.13168/cs.2018.0031 REFRACTORY CERAMICS SYNTHESIS BY SOLID-STATE REACTION BETWEEN CaCO3 (MOLLUSK SHELL) AND Al2O3 POWDERS #JOSÉ G. MIRANDA-HERNÁNDEZ*, MAYAHUEL ORTEGA-AVILÉS**, HÉCTOR HERRERA-HERNÁNDEZ*, CARLOS O. GONZÁLEZ-MORÁN*, GEORGINA GARCÍA-PACHECO***, ENRIQUE ROCHA-RANGEL**** *Universidad Autónoma del Estado de México, Centro Universitario UAEM Valle de México, Laboratorio de Investigación y Desarrollo de Materiales Industriales, Atizapán de Zaragoza, Estado de México, México **Instituto Politécnico Nacional, CNMN, Ciudad de México, México ***Instituto Politécnico Nacional, ESIME TICOMAN, Ciudad de México, México ****Universidad Politécnica de Victoria, Departamento de postgrado, Ciudad Victoria, Tamaulipas, México #E-mail: [email protected] Submitted June 19, 2018; accepted September 11, 2018 Keywords: Refractories, Calcite, Alumina, Snail shells (mollusk shells), Refractory calcium aluminate ceramics, Sintering process, Mechanical properties, Thermal shock resistance Calcium aluminate-based refractory ceramic was developed as an innovative refractory material, using garden snail (Helix aspersa) shells as a natural source of CaCO3. A 1:1 molar ratio mixture of CaCO3 from snail shells and commercial Al2O3 powder was prepared by means of high-energy mechanical milling. The mixed powder was compacted in cylindrical samples (disks) and consolidated by sintering at 1450°C and 1500°C for 1h. The density and porosity were evaluated using the Archimedes principle, while the mechanical properties (hardness, fracture toughness, and shear modulus) were determined by indentation and ultrasonic methods, respectively. The thermal shock resistance was tested by heating samples to temperatures between 900 and 1400°C and subsequent quenching in water at room temperature. X-ray diffraction patterns of sintered samples indicate the formation of different calcium aluminate phases, such as CaAl12O19 (krotite/monoclinic), CaAl4O7 (grossite/monoclinic) and CaAl2O4 (hibonite-5H/hexagonal).
    [Show full text]
  • 2011-09 R&C Newsletter
    Research & Collections Newsletter September 2011 re•search (rī-sûrch′, rē′sûrch) n. 1. Scholarly or scientific investigation or inquiry. See synonyms at inquiry. 2. Close, careful study. 3. When performed on collections, the raison d’être of all great natural history museums. Collection News Dinosaur Institute After more than five years in development, the New Di- nosaur Hall opened its doors to the public on July 16th. The 14,000 square foot Hall features nearly 300 speci- mens, including 20 full skeleton mounts, and includes specimens from the Dinosaur Institute, Vertebrate Pa- leontology, Invertebrate Paleontology, Mineralogy, and Ornithology collections. The project was headed by Luis Chiappe and project manager Jennifer Morgan. The staff of the DI worked on prepping specimens for the exhibit beginning in 2008 with “Thomas” the T. rex. Many of the specimens in the Hall have never before been on display, including the growth series of three T. rex specimens, the full mount of Triceratops, and the excep- tional marine specimens of Platecarpus and Polycotylus. All of the specimens that had been mounted in the old hall, such as the skeletons of Mamenchisaurus, Morenosaurus, Plotosaurus, Camptosaurus, Stegosaurus, Allosaurus, and others, have been restored and re-mounted by Phil Fraley Productions in New Jersey and Pittsburgh and Research Casting International in Ontario. The architectural design of the exhibit was developed by Evidence Design out of New York, and the graphic design was created by KBDA out of Santa Monica. The DI’s Stephanie Abramowicz created much of the artwork seen on the 1 graphic panels on the platforms, and various reconstructions including the post cranial skeleton of the 2-year-old T.
    [Show full text]
  • IMA–CNMNC Approved Mineral Symbols
    Mineralogical Magazine (2021), 85, 291–320 doi:10.1180/mgm.2021.43 Article IMA–CNMNC approved mineral symbols Laurence N. Warr* Institute of Geography and Geology, University of Greifswald, 17487 Greifswald, Germany Abstract Several text symbol lists for common rock-forming minerals have been published over the last 40 years, but no internationally agreed standard has yet been established. This contribution presents the first International Mineralogical Association (IMA) Commission on New Minerals, Nomenclature and Classification (CNMNC) approved collection of 5744 mineral name abbreviations by combining four methods of nomenclature based on the Kretz symbol approach. The collection incorporates 991 previously defined abbreviations for mineral groups and species and presents a further 4753 new symbols that cover all currently listed IMA minerals. Adopting IMA– CNMNC approved symbols is considered a necessary step in standardising abbreviations by employing a system compatible with that used for symbolising the chemical elements. Keywords: nomenclature, mineral names, symbols, abbreviations, groups, species, elements, IMA, CNMNC (Received 28 November 2020; accepted 14 May 2021; Accepted Manuscript published online: 18 May 2021; Associate Editor: Anthony R Kampf) Introduction used collection proposed by Whitney and Evans (2010). Despite the availability of recommended abbreviations for the commonly Using text symbols for abbreviating the scientific names of the studied mineral species, to date < 18% of mineral names recog- chemical elements
    [Show full text]
  • Krotite, Caal2o4, a New Refractory Mineral from the NWA 1934 Meteorite
    American Mineralogist, Volume 96, pages 709–715, 2011 Krotite, CaAl2O4, a new refractory mineral from the NWA 1934 meteorite CHI MA,1,* ANTHONY R. KAMPF,2 HAROLD C. CONNOLLY JR.,3,4,5 JOHN R. BECKETT,1 GEORGE R. ROSSMAN,1 STUART A. SWEENEY SMITH,4,6 AND DEVIN L. SCHRADER5 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, U.S.A. 2Mineral Sciences Department, Natural History Museum of Los Angeles County, Los Angeles, California 90007, U.S.A. 3Department of Physical Sciences, Kingsborough Community College of CUNY, Brooklyn, New York 11235 and Earth and Environmental Sciences, The Graduate Center of CUNY, New York, New York 10024, U.S.A. 4Department of Earth and Planetary Sciences, American Museum of Natural History, New York, New York 10024, U.S.A. 5Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721, U.S.A. 6Department of Geology, Carleton College, Northfield, Minnesota 55057, U.S.A. ABSTRACT Krotite, CaAl2O4, occurs as the dominant phase in an unusual Ca-,Al-rich refractory inclusion from the NWA 1934 CV3 carbonaceous chondrite. Krotite occupies the central and mantle portions of the inclusion along with minor perovskite, gehlenite, hercynite, and Cl-bearing mayenite, and trace hexamolybdenum. A layered rim surrounds the krotite-bearing regions, consisting from inside to outside of grossite, mixed hibonite, and spinel, then gehlenite with an outermost layer composed of Al-rich diopside. Krotite was identified by XRD, SEM-EBSD, micro-Raman, and electron microprobe. The mean chemical composition determined by electron microprobe analysis of krotite is (wt%) Al2O3 63.50, CaO 35.73, sum 99.23, with an empirical formula calculated on the basis of 4 O atoms of Ca1.02Al1.99O4.
    [Show full text]